On the dynamical consequences of the Poynting-Robertson drag caused by solar wind

Details On the dynamical consequences of the Poynting-Robertson drag caused by solar wind On the dynamical consequences of the Poynting-Robertson drag caused by solar wind

Feb 2005

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005dpps.conf..411r&link_type=abstract

Dynamics of Populations of Planetary Systems, Proceedings of IAU Colloquium #197, held 31 August - 4 Spetember, 2004 in Belgrade

Physics

6

Meteoroids, Solar Wind, Methods: Analytical, Celestial Mechanics.

Scientific paper

To correctly take into account the solar wind drag equations for secular variations in the meteoroid orbital semimajor axes and eccentricities were obtained. The equations are similar to those derived for the Poynting- Robertson radiation drag (Wyatt and Whipple 1950). An estimation for the Geminid meteoroid stream shows that the ratios of corpuscular to radiation drags are 0.4 0.7 for particles of size > 10 μm, i.e. the effect is much stronger than was assumed before.

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